Supernova-remnant origin of cosmic rays?

Yousaf M. Butt (), Diego F. Torres, Gustavo E. Romero, Thomas M. Dame and Jorge A. Combi
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Yousaf M. Butt: Harvard-Smithsonian Center for Astrophysics
Diego F. Torres: Jadwin Hall, Princeton University
Gustavo E. Romero: Instituto Argentino de Radioastronomía
Thomas M. Dame: Harvard-Smithsonian Center for Astrophysics
Jorge A. Combi: Instituto Argentino de Radioastronomía

Nature, 2002, vol. 418, issue 6897, 499-499

Abstract: Abstract It is thought that Galactic cosmic-ray nuclei are gradually accelerated to high energies (up to about 300 TeV per nucleon, where 1 TeV is 1012 eV) in the expanding shock waves connected with the remnants of powerful supernova explosions. However, this conjecture has eluded direct observational confirmation1,2 since it was first proposed in 1953 (ref. 3). Enomoto et al.4 claim to have finally found definitive evidence that corroborates this model, proposing that very-high-energy, TeV-range, γ-rays from the supernova remnant (SNR) RX J1713.7 – 3946 are due to the interactions of energetic nuclei in this region. Here we argue that their claim is not supported by the existing multiwavelength spectrum of this source. The search for the origin(s) of Galactic cosmic-ray nuclei may be closing in on the long-suspected supernova-remnant sources, but it is not yet over.

Date: 2002
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DOI: 10.1038/418499a

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